Srg-Siddhinta slow (akan), very sloww(nnadatara), ever (sem¢); also, very swift (¢kghratara), and swift (\ghra). 1B, Of these, the very swift (ti¢ght), that called swift, the slowthe very slow, the even ~-all these five are forms of the motion called direct (j); the somewhat retrograde is retrograde This minute laksification of ahe phRFes of a planet's motion is quite gratuitous, so far as this Siddhanta is concerned, for the terms here given do not once ocer afterward in the text, with the single exception of kwa, which, with its orivatives ix in ot infrequent used to designate retrogradation. Nor does the commentary take the trouble to explain the precise differences of the kind of motion specified. According to MrHoisington (Oriental Astronome! [Tamil and English], Jafna : 1848, p. 188), awagakra is pplied a the notion of a planet when | retr: grading, it passes into a preceding sign. From the classification given in £he second of the two verses it * nbiew thnt kation is initted He cording to the commen%ntor, it is ment to be included among Bhe forms of retrograde motion ; we have conjectured. however, that it might possi bly be used to designate the motion of a planet when, being for the momen) stationary in respeck to longitude, and accordingly either ad. vancing nor retrogading, it is changing its latitude: and we have trans lated the word accordingly 14. By reason of this and bbat rate of motion, from day to day, the planets thus come to an accordance with their observed places (d)—this. their correction (sphttikaraa, I shal care fully explain. Having now disposed of natters of general theory and preliminary explanation, the proper subject of this chapter, the calculation of the true (spatc) from the nean places of the different planets, is ready to be taken up. And the first thing in order is the table of sineE, by aeans of hich all the after calculations are performed. 15. 'The (eight part of the minutes of a sign is called the first sine (); that, increased by the remainder left after sub. tracting from t the puotient arising from dividing it by itself, is the second sine. 16. 'Thus, dividing the tabular sines in succession by the first, and adding to them, in each case, what is left after subtrac ting the quotients from the first, the result is twenty-four tabular sines (g%vyaapinda), in order, as follows:
